Firstly, we concentrated our study of tidal deformability on the isolated non-rotating neutron star case, by using two transition densities \(n_{\mathrm {tr}}=[1.5,2]n_s\)  and eight values of speed of sound bounds \((v_s/c)^2=[1/3,0.4,0.5,0.6,0.7,0.8,0.9,1]\) . The values of transition density were taken to be close to the constraints of Ref. [1]}. The numerical solution of TOV equations' system, by using the previous bounds for sound speed, provided the mass-radius diagram presented in Fig. REF .
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